PANEL (A): Diagram of the net tidal accelerations acting on the planetary surface (caused by the host star’s gravity field).
— astro-ph.EPIn this work, using the simulator VPLanet, we analyze the spin evolution of some selected exoplanets due to the tidal interaction with their host star.
We focus on planets whose spin condition is not obvious, because no study is needed for planets which are undoubtedly fast rotators or undoubtedly trapped rotators; moreover, we consider only exoplanets that are interesting from an astrobiological perspective.
The current spin conditions of the considered planets are hypothesized, taking into account the age of the host star.
Inferences regarding planetary climate and habitability, which is defined by the possibility of stably sustaining the liquid water on the surface, are also discussed.
PANEL (A): Diagram of the net tidal accelerations acting on the planetary surface (caused by the host star’s gravity field). The planet is represented with a top view (i.e., as seen from above). Accelerations are computed in the reference frame of the planetary center. PANEL (B): Representation of the tidal bulge. The planet is represented with a top view. Planetary spinning (black arrow) is counterclockwise, as is the orbital motion around the star (red arrow). — astro-ph.EP
In this work, using the simulator VPLanet, we analyze the spin evolution of some selected exoplanets due to the tidal interaction with their host star.
For a rocky planet, two spin conditions are possible, the trapped rotation and the fast rotation, referring to the cases of achieved and non achieved tidal trapping, respectively.
We focus on planets whose spin condition is not obvious, because no study is needed for planets which are undoubtedly fast rotators or undoubtedly trapped rotators; moreover, we consider only exoplanets that are interesting from an astrobiological perspective. The current spin conditions of the considered planets are hypothesized, taking into account the age of the host star.
Inferences regarding planetary climate and habitability, which is defined by the possibility of stably sustaining the liquid water on the surface, are also discussed. Results of this work show that Kepler-62 f, Kepler-1126 c and Kepler-1544 b are expected to be fast rotators regardless of the orbital eccentricity; the spin condition of Kepler- 186 f, Kepler-62 e, and Kepler-442 b cannot be determined without constraints on the eccentricity, which are currently unavailable; Kepler-440 b is expected to be tidally trapped.
Salvatore Camposeo, Francesco De Paolis, Vincenzo Orofino, Francesco Strafella, Leonardo Di Venere
Subjects: Earth and Planetary Astrophysics (astro-ph.EP)
Cite as: arXiv:2605.11780 [astro-ph.EP] (or arXiv:2605.11780v1 [astro-ph.EP] for this version)
https://doi.org/10.48550/arXiv.2605.11780
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Related DOI:
https://doi.org/10.3390/universe12050140
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Submission history
From: Salvatore Camposeo
[v1] Tue, 12 May 2026 08:48:47 UTC (716 KB)
https://arxiv.org/abs/2605.11780
Astrobiology,
